0 Updated target position for #7 MINNI324 to avoid placing a pair of bright stars at the center of WFC3. 1788139836 ----- Attempting Submission 1 (Thu Sep 14 15:59:47 GMT 2023) ----- HST Phase II Proposal 17440 successfully submitted. Receipt: # 17440-1 ----- Attempting Submission 2 (Thu Sep 21 21:43:03 GMT 2023) ----- Assembling the Milky Way: Adding Globular Clusters from the Sagittarius Dwarf Galaxy Globular clusters (GCs) are important tools to rebuild the accretion history of a galaxy. The newly discovered population of GCs in the main body of the Sagittarius (Sgr) dwarf galaxy can be used to probe this ongoing accretion event onto the Milky Way (MW). We propose to obtain deep WFC3 color-magnitude diagrams, reaching 2-3 magnitudes below the main sequence turn-off, for a dozen of these new Sgr GCs. Our main aim is to measure precise metallicities and ages for these objects, and also derive their structural parameters. The results will allow us to more fully characterize the complete GC system of the infalling Sgr dwarf galaxy, and its ongoing contributions to metallicity distribution, luminosity function, and age-metallicity relations of the Milky Way. This will help paint a detailed picture of galactic cannibalization in our own backyard, a process which continues to shape the Milky Way, and the evolution of galaxies everywhere. We have opted for F606W and F814W for this program because these WFC3 filters have been used in the Treasury Survey of MW GCs and for the current 'missing' clusters program as well. Each of the 12 targets will receive a visit of one orbit. The orbit will be divided into 6 exposures, three in each filter, with the exposure time sequence 10-510-510 for F606W and then 510-510-10 for F814W. The short exposures allow unsaturated photometry of the upper RGB (V~14) in the targets. We have opted for the same exposure times in the two filters because they each reach comparable S/N in equal times for a K0III SED. Our goal is to reach 2-3 magnitudes below the old metal-poor MSTO in the targets to measure the lower main sequence and turnoff regions. Adopting a typical distance of 26.5~kpc, and $A_V \approx 0.25$ the effective $m-M = 17.5$. Scaling from the well-studied Sagittarius GC M54, this puts the MSTO at $V \approx 22$ with $V-I \approx 0.6$, corresponding to a late F-star or early G-star. At 2.5 magnitudes fainter than the MSTO, the color is $\sim 0.8-1.0$, an early to mid K-star with $V=24.5$. The WFC3 ETC shows that WFC3 will reach an optimum S/N of $\gtrsim 40-50$ at 2.5 magnitudes below the MSTO. At the MSTO, both filters reach S/N of $\sim 100$ or better, providing high quality photometry for fitting isochrones and determining cluster properties. We use small dither steps between exposures as it is not necessary to cover the inter-chip gap region, thus all parts of the image receive the full exposure time. Buffer dump limitations, unfortunately, make parallel ACS exposures impossible with the chosen strategy. Elisa Rita Garro has expertise in studies of globular clusters in the Milky Way and the Sagittarius dwarf galaxy. Her work is especially focused on the discovery and characterization of candidate globular clusters to understand their real nature, using a combination of optical and near-IR photometry. She has experience in isochrone fitting to derive the main physical parameters such as reddening, distances, metallicities, and also in construction of projected density and velocity dispersion profiles to obtain structural parameters including concentration indices, and tidal and core radii. Dr. Dante Minniti has a background in stellar astrophysics, stellar populations, star clusters, and variable stars. His expertise is in spectroscopy and multiwavelength photometry, and he is currently PI of the VLT VISTA survey of the Galactic Plane, which includes discovery and characterization of Galactic globular clusters. Dr. Bruno Dias has experience on star clusters, resolved stellar populations, determination of ages, metallicities, distance, extinction using isochrone fitting, structural parameters using radial density profile. He is also leading a spectroscopic follow up of recently discovered globular clusters with VVV survey, and is expert in analyzing MUSE IFU data. Dr. Michael Gregg has extensive expertise in planning and executing HST programs, in reducing WFC3 and ACS data using drizzling, and in the PSF photometry analysis of the resulting images. He has a background in galaxy clusters, tidal disruption of galaxies, globular clusters in early type galaxies, ultra-compact dwarf galaxies, and resolved star photometry of red giant branch populations. He will take main responsibility for planning the Phase II proposal and the drizzling reductions, plus collaborating in subsequent aspects of the photometry and interpretation and modeling of the color magnitude diagrams. Francesca Lucertini has expertise in reducing WFC3 and ACS data to obtain multiwavelength astro-photometric catalogs. She has a background in stellar astrophysics, globular clusters, multiple stellar populations, and determination of stellar populations ages. She also has expertise in high-resolution spectroscopy and chemical characterization of stars. Dr. Maren Hempel has a background on Globular Cluster systems, mostly extragalactic (where GCs appear as point sources). She also worked on NICMOS data in resolved M33 Globular Clusters. She also has expertise on photometric completeness, especially in the near-IR, i.e. VVV data. 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